High Energy Astrophysical Phenomena

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New submissions for Thu, 9 May 24

[1]  arXiv:2405.04574 [pdf, other]

Title: The Orbit of NGC 5907 ULX-1

Authors: Andrea Belfiore (1), Ruben Salvaterra (1), Lara Sidoli (1), Gian Luca Israel (2), Luigi Stella (2), Andrea De Luca (1), Sandro Mereghetti (1), Paolo Esposito (3, 1), Fabio Pintore (4), Antonino D'Aì (4), Guillermo Rodrìguez Castillo (4), Dominic J. Walton (5, 6), Felix Fürst (7), Danilo Magistrali (8), Anna Wolter (9), Matteo Imbrogno (10, 2, 11) ((1) INAF IASF-Mi, (2) INAF OAR, (3) IUSS Pavia, (4) INAF IASF-Pa, (5) Centre for Astrophysics Research University of Hertfordshire, (6) Institute of Astronomy University of Cambridge, (7) ESA ESAC, (8) Universidad Pontificia Comillas, (9) INAF OAB, (10) Dipartimento di Fisica Università Tor Vergata, (11) Università La Sapienza)

Comments: 11 pages, 2 tables, 6 figures

Journal-ref: ApJ 965, 78B (2024)

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We report on the orbit of the binary system powering the most extreme ultraluminous X-ray pulsar known to date: NGC 5907 ULX-1 (hereafter ULX1). ULX1 has been the target of a substantial multi-instrument campaign, mainly in the X-ray band, but no clear counterparts are known in other bands. Although ULX1 is highly variable and pulsations can be transient (regardless of the source flux), the timing data collected so far allow us to investigate the orbit of this system. We find an orbital period $P_{orb}=5.7^{+0.1}_{-0.6}\text{ d}$ and a projected semi-axis $A_1 =3.1^{+0.8}_{-0.9}\text{ lts}$. The most likely ephemeris is: $P_{orb}=5.6585(6)\text{ d}$, $A_1 = 3.1(4)\text{ lts}$, and the epoch of ascending nodes passage is: $T_{asc} = 57751.37(5)\text{ MJD}$. However, there are 6 similar solutions, acceptable within $3\,\sigma$. We find further indications that ULX1 is a high-mass X-ray binary. This implies that we are observing its orbit face-on, with an inclination $<5\text{ deg}$.

[2]  arXiv:2405.04583 [pdf, other]

Title: SN2023fyq: A Type Ibn Supernova With Long-standing Precursor Activity Due to Binary Interaction

Authors: Yize Dong, Daichi Tsuna, Stefano Valenti, David J. Sand, Jennifer E. Andrews, K. Azalee Bostroem, Griffin Hosseinzadeh, Emily Hoang, Saurabh W. Jha, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolas E. Meza Retamal, Jeniveve Pearson, Manisha Shrestha, Alceste Bonanos, D. Andrew Howell, Nathan Smith, Joseph Farah, Daichi Hiramatsu, Koichi Itagaki, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Emmanouela N. Paraskeva, Craig Pellegrino, Giacomo Terreran, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart

Comments: submitted to ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

We present photometric and spectroscopic observations of SN 2023fyq, a type Ibn supernova in the nearby galaxy NGC 4388 (D$\simeq$18~Mpc). In addition, we trace long-standing precursor emission at the position of SN 2023fyq using data from DLT40, ATLAS, ZTF, ASAS-SN, Swift, and amateur astronomer Koichi Itagaki. Precursor activity is observed up to nearly three years before the supernova explosion, with a relatively rapid rise in the final 100 days. The double-peaked post-explosion light curve reaches a luminosity of $\sim10^{43}~\rm erg\,s^{-1}$. The strong intermediate-width He lines observed in the nebular spectrum of SN 2023fyq imply the interaction is still active at late phases. We found that the precursor activity in SN 2023fyq is best explained by the mass transfer in a binary system involving a low-mass He star and a compact companion. An equatorial disk is likely formed in this process ($\sim$0.6$\rm M_{\odot}$), and the interaction of SN ejecta with this disk powers the main peak of the supernova. The early SN light curve reveals the presence of dense extended material ($\sim$0.3$\rm M_{\odot}$) at $\sim$3000$\rm R_{\odot}$ ejected weeks before the SN explosion, likely due to final-stage core silicon burning or runaway mass transfer resulting from binary orbital shrinking, leading to rapid rising precursor emission within $\sim$30 days prior to explosion. The final explosion could be triggered either by the core-collapse of the He star or by the merger of the He star with a compact object. SN 2023fyq, along with SN 2018gjx and SN 2015G, forms a unique class of Type Ibn SNe which originate in binary systems and are likely to exhibit detectable long-lasting pre-explosion outbursts with magnitudes ranging from $-$10 to $-$13.

[3]  arXiv:2405.04626 [pdf, other]

Title: An arcsecond view at 1-2 GHz into the Galactic Bulge

Authors: E. C. Pattie, T. J. Maccarone (Texas Tech University), C. T. Britt (STScI), C. O. Heinke (University of Alberta), P. G. Jonker (SRON, Radboud University), D. R. Lorimer (WVU), G. R. Sivakoff (University of Alberta), D. Steeghs (University of Warwick), J. Strader (Michigan State University), M. A. P. Torres (IAC, University of La Laguna), R. Wijnands (Amsterdam)

Comments: 20 pages, 13 figures. Accepted for publication in MNRAS

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)

We present the results of a high angular resolution (1.1") and sensitivity (maximum of ~0.1 mJy) radio survey at 1-2 GHz in the Galactic Bulge. This complements the X-ray Chandra Galactic Bulge Survey, and investigates the full radio source population in this dense Galactic region. Radio counterparts to sources at other wavelengths can aid in classification, as there are relatively few types of objects that are reasonably detectable in radio at kiloparsec distances, and even fewer that are detected in both X-rays and radio. This survey covers about 3 square degrees of the Galactic Bulge Survey area (spanning the Galactic coordinate range of -3deg < l < +3deg and +1.6deg < b < +2.1deg as a first look into this region of the Galaxy with this combination of frequency, resolution, and sensitivity. Spectral indices within the observed band of 1-2 GHz were calculated for each source to assist in determining its emission mechanism. We find 1617 unique sources in the survey, 25 of which are radio counterparts to X-ray sources, and about 100 of which are steep-spectrum (alpha <~ -1.4) point sources that are viable pulsar candidates. Four radio sources are of particular interest: a compact binary; an infrared transient with an inverted radio spectrum; a potential transitional millisecond pulsar candidate; and a very steep spectrum radio source with an X-ray and bright infrared counterpart. We discuss other notable sources, including possible radio transients, potential new planetary nebulae, and active galactic nuclei.

[4]  arXiv:2405.04749 [pdf, other]

Title: Bayesian Black Hole Photogrammetry

Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We propose a simple, analytic dual-cone accretion model for horizon scale images of the cores of Low-Luminosity Active Galactic Nuclei (LLAGN), including those observed by the Event Horizon Telescope (EHT). Our underlying model is of synchrotron emission from an axisymmetric, magnetized plasma, which is constrained to flow within two oppositely oriented cones that are aligned with the black hole's spin axis. We show that this model can accurately reproduce images for a variety of time-averaged general relativistic magnetohydrodynamic (GRMHD) simulations, that it accurately recovers both the black hole and emission parameters from these simulations, and that it is sufficiently efficient to be used to measure these parameters in a Bayesian inference framework with radio interferometric data. We show that non-trivial topologies in the source image can result in non-trivial multi-modal solutions when applied to observations from a sparse array, such as the EHT 2017 observations of M87${}^*$. The presence of these degeneracies underscores the importance of employing Bayesian techniques that adequately sample the posterior space for the interpretation of EHT measurements. We fit our model to the EHT observations of M87${}^*$ and find a 95% Highest Posterior Density Interval (HPDI) for the mass-to-distance ratio of $\theta_g\in(2.84,3.75)\,\mu{\rm as}$, and give an inclination of $\theta_{\rm o}\in(11^\circ,24^\circ)$. These new measurements are consistent with mass measurements from the EHT and stellar dynamical estimates (e.g., Gebhardt et al. 2011; EHTC et al. 2019a,b; Liepold et al. 2023), and with the spin axis inclination inferred from properties of the M87${}^*$ jet (e.g., Walker et al. 2018).

[5]  arXiv:2405.04802 [pdf, other]

Title: The Northern Cross Fast Radio Burst project IV. Multiwavelength study of the actively repeating FRB 20220912A

Authors: D. Pelliciari, G. Bernardi, M. Pilia, G. Naldi, G. Maccaferri, F. Verrecchia, C. Casentini, M. Perri, F. Kirsten, G. Bianchi, C. Bortolotti, L. Bruno, D. Dallacasa, P. Esposito, A. Geminardi, S. Giarratana, M. Giroletti, R. Lulli, A. Maccaferri, A. Magro, A. Mattana, F. Perini, G. Pupillo, M. Roma, M. Schiaffino, G. Setti, M. Tavani, M. Trudu, A. Zanichelli

Comments: submitted to A&A, 13 pages

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

Fast radio bursts (FRBs) are energetic, millisecond-duration radio pulses observed at extragalactic distances and whose origin is still largely debated. A fraction of the FRB population have shown repeating bursts. It is still unclear whether these represent a distinct class of sources. We investigate the bursting behaviour of FRB 20220912A, one of the most active repeating FRBs known. In particular, we focus on its burst energy distribution, linked to the source energetics, and its emission spectrum, the latter directly related to the underlying emission mechanism. We monitored FRB 20220912A at $408$ MHz with the Northern Cross radio telescope and at $1.4$ GHz using the $32$-m Medicina Grueff radio telescope. Additionaly, we conducted $1.2$ GHz observations taken with the upgraded-Giant Meter Wave Radio Telescope searching for a persistent radio source coincident with FRB 20220912A, and we present the first upper limits obtained from a monitoring in X and $\gamma$ rays conducted with Swift and AGILE satellites. We report 16 new bursts from FRB 20220912A at $408$ MHz during the period of time between October 16$^{\rm th}$ 2022 and December 31$^{\rm st}$ 2023. Their cumulative spectral energy distribution follows a power law with slope $\alpha_E = -1.5 \pm 0.3$ and we measure a repetition rate of $0.15 \pm 0.04$ hr$^{-1}$ for bursts having fluence $\mathcal{F} \geq 20$ Jy ms. Furthermore, we report no detections at $1.4$ GHz during down to a fluence of $\mathcal{F} \geq 13$ Jy ms. These non-detections imply an upper limit of $\beta < -2.3$, with $\beta$ being the global spectral index of FRB 20220912A. This is inconsistent with positive $\beta$ values found for the only two known cases in which an FRB has been detected in separate spectral bands. We find that FRB 20220912A has shown a decline of $4$ orders of magnitude in its bursting activity at $1.4$ GHz over a one year ... (abridged)

[6]  arXiv:2405.04898 [pdf, other]

Title: A Gamma-ray Emitting Collisional Ring Galaxy System in our Galactic Neighborhood

Authors: Vaidehi S. Paliya, D. J. Saikia (IUCAA)

Comments: ApJ Letters, in press

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA)

The astrophysical $\gamma$-ray photons carry the signatures of the violent phenomena happening on various astronomical scales in our Universe. This includes supernova remnants, pulsars, and pulsar wind nebulae in the Galactic environment and extragalactic relativistic jets associated with active galactic nuclei (AGN). However, $\sim$30\% of the \gm-ray sources detected with the Fermi Large Area Telescope lack multiwavelength counterpart association, precluding us from characterizing their origin. Here we report, for the first time, the association of a collisional ring galaxy system in our Galactic neighborhood (distance $\sim$10 Mpc), formed as a consequence of a smaller `bullet' galaxy piercing through a larger galaxy, as the multi-frequency counterpart of an unassociated $\gamma$-ray source 4FGL~J1647.5$-$5724. The system, also known as "Kathryn's Wheel", contains two dwarf irregular galaxies and an edge-on, late-type, spiral galaxy surrounded by a ring of star-forming knots. We utilized observations taken from the Neil Gehrels Swift observatory, Rapid ASKAP Continuum Survey, SuperCOSMOS H$\alpha$ Survey, Dark Energy Survey, and Visible MultiObject Spectrograph at Very Large Telescope to ascertain the association with 4FGL~J1647.5$-$5724 and to explore the connection between the star-forming activities and the observed $\gamma$-ray emission. We found that star-formation alone cannot explain the observed $\gamma$-ray emission, and additional contribution likely from the pulsars/supernova remnants or buried AGN is required. We conclude that arcsecond/sub-arcsecond-scale observations of this extraordinary $\gamma$-ray emitting galaxy collision will be needed to resolve the environment and explore the origin of cosmic rays.

[7]  arXiv:2405.04908 [pdf, other]

Title: Sedimentary rocks from Mediterranean drought in the Messinian age as a probe of the past cosmic ray flux

Authors: Lorenzo Caccianiga, Claudio Galelli, Lorenzo Apollonio, Federico Maria Mariani, Paolo Magnani, Alessandro Veutro

Comments: 6 pages, 2 figures. To be submitted to PRX

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Geophysics (physics.geo-ph)

We propose the use of natural minerals as detectors to study the past flux of cosmic rays. This novel application of the \textit{paleo-detector} technique requires a specific approach as it needs samples that have been exposed to secondary cosmic rays for a well defined period of time. We suggest here the use of the evaporites formed during the desiccation of the Mediterranean sea ${\sim}6$ Myr ago. These minerals have been created and exposed to the air or under a shallow water basin for ${\sim}500$ kyr before being quickly submerged again by a km-scale overburden of water. We show that, by looking at the damages left in the minerals by muons in cosmic ray showers, we could detect differences in the primary cosmic ray flux during that period, as the ones expected from nearby supernova explosions, below the percent-level. We show also that little to no background from radioactive contamination and other astroparticles is expected for this kind of analysis.

[8]  arXiv:2405.04935 [pdf, other]

Title: A high-resolution radio morphology and polarization of the kpc-scale X-ray jet of PKS 1127-145

Authors: M. Orienti, A. Siemiginowska, F. D'Ammando, G. Migliori

Comments: 10 pages, 8 figures, accepted for publication in A&A

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We report on new multi-frequency Very Large Array (VLA) radio observations and Chandra X-ray observations of a radio-loud quasar with a ~300 kpc long jet, PKS 1127-145, during a flaring event detected in $\gamma$-rays by the Fermi Large Area Telescope in 2020 December. The high angular resolution of the new radio images allows us to disentangle for the first time the inner kpc-scale jet from the core contribution. The inner radio jet, up to 15 kpc from the core, is highly polarized (33 per cent) and the magnetic field is parallel to the jet axis. At about 18 arcsec from the core the jet slightly bends and we observe a re-brightening of the radio emission and a 90-degree rotation of the magnetic field, likely highlighting the presence of a shock that is compressing the magnetic field to a plane perpendicular to the jet axis and where efficient particle acceleration takes place. At the same position the X-ray emission fades, suggesting a deceleration of the bulk velocity of the jet after the bend. A change in velocity and collimation of the jet is supported by the widening of the jet profile and the detection of a limb-brightened structure connecting the bending region with the jet termination. The limb-brightened structure might indicate the co-existence of both longitudinal and transverse velocity gradients at the jet bending. There is no evidence for significant brightening of the kpc-scale jet in the radio or X-ray band during the $\gamma$-ray flare. The X-ray flux, $F_{\rm 2-10\,keV} =
(6.24\pm0.57)\times10^{-12}$ ergs s$^{-1}$ cm$^{-2}$, measured by Chandra from the quasar core is consistent with the flux measured by the X-Ray Telescope on board the Neil Gehrels Swift Observatory after the high-energy flare. Our results indicate that the $\gamma$-ray flaring region is located within the VLA source core.

[9]  arXiv:2405.04981 [pdf, other]

Title: A unified theory of the self-similar supersonic Marshak wave problem

Authors: Menahem Krief, Ryan G. McClarren

Comments: Accepted for publications in Physics of Fluids

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Mathematical Physics (math-ph); Computational Physics (physics.comp-ph); Fluid Dynamics (physics.flu-dyn); Plasma Physics (physics.plasm-ph)

We present a systematic study of the similarity solutions for the Marshak wave problem, in the local thermodynamic equilibrium (LTE) diffusion approximation and in the supersonic regime. Self-similar solutions exist for a temporal power law surface temperature drive and a material model with power law temperature dependent opacity and energy density. The properties of the solutions in both linear and nonlinear conduction regimes are studied as a function of the temporal drive, opacity and energy density exponents. We show that there exists a range of the temporal exponent for which the total energy in the system decreases, and the solution has a local maxima. For nonlinear conduction, we specify the conditions on the opacity and energy density exponents under which the heat front is linear or even flat, and does posses its common sharp character; this character is independent of the drive exponent. We specify the values of the temporal exponents for which analytical solutions exist and employ the Hammer-Rosen perturbation theory to obtain highly accurate approximate solutions, which are parameterized using only two numerically fitted quantities. The solutions are used to construct a set of benchmarks for supersonic LTE radiative heat transfer, including some with unusual and interesting properties such as local maxima and non sharp fronts. The solutions are compared in detail to implicit Monte-Carlo and discrete-ordinate transport simulations as well gray diffusion simulations, showing a good agreement, which highlights their usefulness as a verification test problem for radiative transfer simulations.

[10]  arXiv:2405.05120 [pdf, ps, other]

Title: GRB afterglows with energy injections in AGN accretion disks

Authors: Bao-Quan Huang, Tong Liu, Xiao-Yan Li, Yun-Feng Wei

Comments: 12 pages, 6 figures, 2 tables, accepted for publication in ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

Active galactic nucleus (AGN) disks are widely considered potential hosts for various high-energy transients, including gamma-ray bursts (GRBs). The reactivation of GRB central engines can provide additional energy to shocks formed during the interaction of the initially ejected GRB jets with the circumburst material, commonly referred to as energy injections. In this paper, we study GRBs occurring in AGN disks within the context of energy injections. We adopt the standard external forward shock (EFS) model and consider both short- and long-duration GRB scenarios. Light curves for two types of radiation, namely the radiation from the heated disk material (RHDM) and GRB afterglows, are computed. We find that the energy injection facilitates the EFS to break out from the photosphere of the low-density AGN disk at relativistic velocity. Moreover, the energy injection almost does not affect the RHDM but significantly enhances the peak flux of the GRB afterglows.

[11]  arXiv:2405.05221 [pdf, other]

Title: XMM-Newton observations of the extragalactic microquasar S26 and their implications for PeV cosmic rays

Authors: L. Abaroa, G.E. Romero, G.C. Mancuso, F.N. Rizzo

Comments: 6 pages, 2 figures, accepted for publication in Proceedings of Science (HEPRO conference)

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

The extragalactic microquasar S26 has the most powerful jets observed in accreting binaries, with a kinetic luminosity of $L_{\rm jet}\sim10^{40}\,{\rm erg\,s^{-1}}$. According to the jet-disk symbiosis model, this implies that the accretion power to the stellar black hole at the core of the system should be very super-Eddington, on the order of $L_{\rm acc}\sim L_{\rm jet}$. However, the observed X-ray flux of this system, measured by the \textit{Chandra} and \textit{XMM-Newton} telescopes, indicates an apparent very sub-Eddington accretion luminosity of $L_{\rm X}\approx 10^{37}\,{\rm erg\,s^{-1}}$, orders of magnitude smaller than the jet power. We present here a preliminary investigation of the relationship between jet and disk power, analyze an X-ray observation of S26 obtained with \textit{XMM-Newton}, and propose an explanation for the emission. We also examine the acceleration and distribution of the particles to discuss the feasibility of microquasars as potential PeVatron sources, exploring their ability to produce cosmic rays with energies of about 1 PeV or higher.

[12]  arXiv:2405.05247 [pdf, other]

Title: Neutrinos and gamma rays from beta decays in an active galactic nucleus NGC 1068 jet

Authors: Koichiro Yasuda, Yoshiyuki Inoue, Alexander Kusenko

Comments: 4 pages, 1 figure

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

We show that TeV neutrinos detected from the nearby active galaxy NGC 1068 can be explained by the beta decays of neutrons produced in photodisintegration of nuclei on ultraviolet photons in the jet. The photodisintergation of nuclei occurs at energies above a few PeV, which explains the 1-100 TeV energies of the observed neutrinos. The gamma-ray flux accompanying the beta decays is expected to be much lower than the neutrino flux, and it agrees well with the gamma-ray observations of NGC 1068. This scenario can be applicable to other jetted Seyfert galaxies such as NGC 4151. The flavor ratio studies could be a test of this beta decay jet scenario for gamma-ray deficit neutrino sources.

Cross-lists for Thu, 9 May 24

[13]  arXiv:2405.04568 (cross-list from hep-ph) [pdf, other]

Title: Relic Neutrino Background from Cosmic-Ray Reservoirs

Authors: Andrea Giovanni De Marchi, Alessandro Granelli, Jacopo Nava, Filippo Sala

Comments: 5 pages + appendices, 5 figures, 1 table

Subjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE)

We compute the flux of relic neutrino background (R$\nu$B) up-scattered by ultra-high-energy (UHE) cosmic rays (CRs) in clusters that act as CR-reservoirs. The long trapping times of UHECRs make this flux larger than that of R$\nu$B up-scattered by UHECRs on their way to Earth, which we also compute. We find that IceCube excludes R$\nu$B weighted overdensities larger than $10^{10}$ in clusters, and that PUEO, RNO-G, GRAND and IceCube-Gen2 will test values down to $10^{8}$. Our treatment incorporates the momentum transfer dependence of the neutrino-nucleus cross section, deep inelastic scattering, a mixed UHECR composition, and flavour information on the up-scattered R$\nu$B fluxes for both cases of neutrino mass spectrum with normal and inverted ordering, providing new handles to possibly disentangle the up-scattered R$\nu$B from cosmogenic neutrinos.

[14]  arXiv:2405.04647 (cross-list from physics.space-ph) [pdf, other]

Title: First direct observations of interplanetary shock impact angle effects on actual geomagnetically induced currents: The case of the Finnish natural gas pipeline system

Authors: Denny M. Oliveira, Eftyhia Zesta, Sergio Vidal-Luengo

Comments: 29 pages, 9 figures

Journal-ref: Frontiers in Astronomy and Space Science (2024)

Subjects: Space Physics (physics.space-ph); Earth and Planetary Astrophysics (astro-ph.EP); High Energy Astrophysical Phenomena (astro-ph.HE); Atmospheric and Oceanic Physics (physics.ao-ph)

The impact of interplanetary (IP) shocks on the Earth's magnetosphere can greatly disturb the geomagnetic field and electric currents in the magnetosphere-ionosphere system. At high latitudes, the current systems most affected by the shocks are the auroral electrojet currents. These currents then generate ground geomagnetically induced currents (GICs) that couple with and are highly detrimental to ground artificial conductors including power transmission lines, oil/gas pipelines, railways, and submarine cables. Recent research has shown that the shock impact angle, the angle the shock normal vector performs with the Sun-Earth line, plays a major role in controlling the subsequent geomagnetic activity. More specifically, due to more symmetric magnetospheric compressions, nearly frontal shocks are usually more geoeffective than highly inclined shocks. In this study, we utilize a subset (332 events) of a shock list with more than 600 events to investigate, for the first time, shock impact angle effects on the subsequent GICs right after shock impact (compression effects) and several minutes after shock impact (substorm-like effects). We use GIC recordings from the Finnish natural gas pipeline performed near the M\"ants\"al\"a compression station in southern Finland. We find that GIC peaks (> 5 A) occurring after shock impacts are mostly caused by nearly frontal shocks and occur in the post-noon/dusk magnetic local time sector. These GIC peaks are presumably triggered by partial ring current intensifications in the dusk sector. On the other hand, more intense GIC peaks (> 20 A) generally occur several minutes after shock impacts and are located around the magnetic midnight terminator. These GIC peaks are most likely caused by intense energetic particle injections from the magnetotail which frequently occur during substorms.

[15]  arXiv:2405.04653 (cross-list from gr-qc) [pdf, other]

Title: Nonradial instabilities in anisotropic neutron stars

Authors: Shu Yan Lau, Siddarth Ajith, Victor Guedes, Kent Yagi

Comments: 7+7 pages, 2+1 figures, submitted to PRL

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

Non-radial oscillation modes of a neutron star possess valuable information about its internal structure and nuclear physics. Starting from the quadrupolar order, such modes under general relativity are known as quasi-normal modes since they dissipate energy through gravitational radiation and their frequencies are complex. The stability of these modes is governed by the sign of the imaginary part of the frequency, which determines whether the mode would decay or grow over time. In this Letter, we develop a fully consistent framework in general relativity to study quasi-normal modes of neutron stars with anisotropic pressure, whose motivation includes strong internal magnetic fields and non-vanishing shear or viscosity. We employ parametrized models for the anisotropy and solve the perturbed Einstein field equations numerically. We find that, unlike the case for isotropic neutron stars, the imaginary parts of some of the pressure ($p$-)modes flip signs as the degree of anisotropy deviates from zero, depicting a transition from stable modes to unstable modes. This finding indicates that some anisotropic neutron star models are unstable, potentially restricting the form of sustained anisotropy.

[16]  arXiv:2405.04690 (cross-list from gr-qc) [pdf, other]

Title: An efficient GPU-accelerated multi-source global fit pipeline for LISA data analysis

Authors: Michael L. Katz, Nikolaos Karnesis, Natalia Korsakova, Jonathan R. Gair, Nikolaos Stergioulas

Comments: 25 pages, 6 figures

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE); Instrumentation and Methods for Astrophysics (astro-ph.IM)

The large-scale analysis task of deciphering gravitational wave signals in the LISA data stream will be difficult, requiring a large amount of computational resources and extensive development of computational methods. Its high dimensionality, multiple model types, and complicated noise profile require a global fit to all parameters and input models simultaneously. In this work, we detail our global fit algorithm, called "Erebor," designed to accomplish this challenging task. It is capable of analysing current state-of-the-art datasets and then growing into the future as more pieces of the pipeline are completed and added. We describe our pipeline strategy, the algorithmic setup, and the results from our analysis of the LDC2A Sangria dataset, which contains Massive Black Hole Binaries, compact Galactic Binaries, and a parameterized noise spectrum whose parameters are unknown to the user. We recover posterior distributions for all 15 (6) of the injected MBHBs in the LDC2A training (hidden) dataset. We catalog $\sim12000$ Galactic Binaries ($\sim8000$ as high confidence detections) for both the training and hidden datasets. All of the sources and their posterior distributions are provided in publicly available catalogs.

[17]  arXiv:2405.04833 (cross-list from gr-qc) [pdf, ps, other]

Title: Thermal analysis of black hole in de Rham--Gabadadze--Tolley massive gravity in Barrow entropy framework

Authors: Muhammad Yasir, Tiecheng Xia, Sudhaker Upadhyay

Comments: 19 pages, 18 captioned figures, published in Physica Scripta

Journal-ref: Phys. Scr. 99 (2024) 065003

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Theory (hep-th)

This study examines a recently hypothesized black hole solution in de Rham--Gabadadze--Tolley massive gravity. Firstly, we consider the negative cosmological constant as a thermodynamic pressure. We extract the thermodynamical properties such as Hawking temperature, heat capacity and Gibbs free energy using the Barrow entropy. We also obtain a new pressure associated to the perfect fluid dark matter and discuss the first-order van der Waals-like phase transition. This black hole's stability is investigated through specific heat and Gibbs free energy. Also, we analyze the thermodynamic curvatures behavior of black hole through geometry methods (Weinhold, Ruppeiner, Hendi-Panahiyah-Eslam-Momennia (HPEM), and geometrothermodynamics (GTD)).

[18]  arXiv:2405.05038 (cross-list from gr-qc) [pdf, other]

Title: Bounds on the charge of the graviton using gravitational wave observations

Authors: Sreejith Nair, Aditya Vijaykumar, Sudipta Sarkar

Comments: 9 pages, 3 figures

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph); High Energy Physics - Theory (hep-th)

If the graviton possesses a non-zero charge $q_g$, gravitational waves (GW) originating from astrophysical sources would experience an additional time delay due to intergalactic magnetic fields. This would result in a modification of the phase evolution of the observed GW signal similar to the effect induced by a massive graviton. As a result, we can reinterpret the most recent upper limits on the graviton's mass as constraints on the joint mass-charge parameter space, finding $|q_g|/{e} < 3\times 10^{-34}$ where $e$ represents the charge of an electron. Additionally, we illustrate that a charged graviton would introduce a constant phase difference in the gravitational waves detected by two spatially separated GW detectors due to the Aharonov-Bohm effect. Using the non-observation of such a phase difference for the GW event GW190814, we establish a mass-independent constraint $|q_g|/e < 2\times 10^{-26}$. To the best of our knowledge, our results constitute the first-ever bounds on the charge of the graviton. We also discuss various caveats involved in our measurements and prospects for strengthening these bounds with future GW observations.

[19]  arXiv:2405.05094 (cross-list from gr-qc) [pdf, other]

Title: Mass function of stellar black holes as revealed by the LIGO-Virgo-KAGRA observations

Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu

Comments: 14 pages, 5 figures, 1 table

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

Ninety gravitational wave events have been detected by the LIGO-Virgo-KAGRA network and are released in the Gravitational-Wave Transient Catalog. Among these events, 83 cases are definitely binary black hole mergers since the masses of all the objects involved significantly exceed the upper limit of neutron stars. The black holes in these merger events naturally form two interesting samples, a pre-merger sample that includes all the black holes before the mergers and a post-merger sample that consists of the black holes generated during the merging processes. The former represents black holes that once existed in the Universe, while the latter represents newly born black holes. Here we present a statistical analysis on these two samples. The non-parametric $\tau$ statistic method is adopted to correct for the observational selection effect. The Lynden-Bell's $C^{-}$ method is further applied to derive the mass distribution and density function of black holes. It is found that the mass distribution can be expressed as a broken power-law function. More interestingly, the power-law index in the high mass region is comparable for the two samples. The number density of black holes is found to depend on redshift as $\rho(z) \propto z^{-2.06}$-$z^{-2.12}$ based on the two samples. Implications of these findings on the origin of black holes are discussed.

[20]  arXiv:2405.05127 (cross-list from astro-ph.SR) [pdf, other]

Title: Evolution of Spin in the Intermediate Polar CC Sculptoris

Authors: John A. Paice, S. Scaringi, N. Castro Segura, A. Sahu, K. Ilkiewicz, Deanne L. Coppejans, D. De Martino, C. Knigge, M. Veresvarska

Comments: 5 pages, 6 figures. Accepted into MNRAS Letters

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); High Energy Astrophysical Phenomena (astro-ph.HE)

We report on spin variations in the intermediate polar and cataclysmic variable CC Scl, as seen by the Transiting Exoplanet Survey Satellite (TESS). By studying both the spin period and its harmonic, we find that the spin has varied since it was first observed in 2011. We find the latest spin value for the source to be 389.473(6)s, equivalent to 0.00450779(7) days, 0.02s shorter than the first value measured. A linear fit to these and intermediate data give a rate of change of spin ~-4.26(2.66)e10^-11 and a characteristic timescale tau~2.90e10^5 years, in line with other known intermediate polars with varying spin. The spin profile of this source also matches theoretical spin profiles of high-inclination intermediate polars, and furthermore, appears to have changed in shape over a period of three years. Such `spin-up' in an intermediate polar is considered to be from mass accretion onto the white dwarf (the primary), and we note the presence of dwarf nova eruptions in this source as being a possible catalyst of the variations.

Replacements for Thu, 9 May 24

[21]  arXiv:2212.06166 (replaced) [pdf, other]

Title: Rapid determination of LISA sensitivity to extreme mass ratio inspirals with machine learning

Authors: Christian E. A. Chapman-Bird, Christopher P. L. Berry, Graham Woan

Comments: 12 pages, 4 figures; changes to match published version

Journal-ref: MNRAS 522(4), 6043-6054 (2023)

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

[22]  arXiv:2303.16775 (replaced) [pdf, other]

Title: Fast radio burst energy function in the presence of $\rm DM_{host}$ variation

Authors: Ji-Guo Zhang, Yichao Li, Jia-Ming Zou, Ze-Wei Zhao, Jing-Fei Zhang, Xin Zhang

Comments: 15 pages, 5 figures; published version

Journal-ref: Universe 2024, 10(5), 207

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph)

[23]  arXiv:2312.16859 (replaced) [pdf, other]

Title: Accretion flows around spinning compact objects in the post-Newtonian regime

Authors: Elham Nazari, Samik Mitra, Shahram Abbassi, Santabrata Das

Comments: 42 pages, 9 figures, and 5 appendices, Accepted for publication in JCAP

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

[24]  arXiv:2402.08402 (replaced) [pdf, other]

Title: Enhanced Blandford Znajek Jet in Loop Quantum Black Hole

Authors: Hong-Xuan Jiang, Indu K. Dihingia, Cheng Liu, Yosuke Mizuno, Tao Zhu

Comments: 14 pages, 5 figures. A JCAP. Accepted by JCAP

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

[25]  arXiv:2402.19314 (replaced) [pdf, other]

Title: Sources of high-energy astrophysical neutrinos

Authors: Walter Winter

Comments: Invited talk given at the High Energy Phenomena in Relativistic Outflows VIII (HEPROVIII) conference, 23-26 October, 2023, Paris, France

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[26]  arXiv:2403.16074 (replaced) [pdf, ps, other]

Title: Finding Candidate TeV Halos among Very-High Energy Sources

Authors: Dong Zheng, Zhongxiang Wang (Yunnan University)

Comments: 15 pages, 7 figures, 4 tables, referee's comments incorporated, accepted for publication in ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[27]  arXiv:2403.16889 (replaced) [pdf, other]

Title: Quantitative modelling of type Ia supernovae spectral time series: Constraining the explosion physics

Authors: M. R. Magee, L. Siebenaler, K. Maguire, K. Ackley, T. Killestein

Comments: 28 pages, 4 appendices, 18 figures, 4 tables. Accepted for publication in MNRAS. The riddler code is publicly available at this https URL

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

[28]  arXiv:2404.03237 (replaced) [pdf, other]

Title: Dynamics and Emission Properties of Flux Ropes from Two-Temperature GRMHD Simulations with Multiple Magnetic Loops

Authors: Hong-Xuan Jiang, Yosuke Mizuno, Indu K. Dihingia, Antonios Nathanail, Ziri Younsi, Christian M. Fromm

Comments: 14 pages, 17 figures. Accepted by A&A

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[29]  arXiv:2405.00769 (replaced) [pdf, other]

Title: Simple fits for the neutrino luminosities from protoneutron star cooling

Authors: Giuseppe Lucente (1,2,3,4), Malte Heinlein (5,6), H.-Thomas Janka (5), Alessandro Mirizzi (1,2) ((1) University of Bari, (2) INFN Bari, (3) KIP, Heidelberg, (4) ITP, Heidelberg, (5) MPI for Astrophysics, Garching, (6) TUM School of Nat. Sciences, Garching)

Comments: 30 pages, 16 figures, 11 tables. Minor changes, additional references included

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

[30]  arXiv:2405.01672 (replaced) [pdf, other]

Title: Multi-filter UV to NIR Data-driven Light Curve Templates for Stripped Envelope Supernovae

Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard

Comments: 65 pages, 35 images, 8 tables, submitted to The Astrophysical Journal Supplement Series

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

[31]  arXiv:2405.02658 (replaced) [pdf, other]

Title: Modeling Hadronic Interactions in Ultra-High-Energy Cosmic Rays within Astrophysical Environments: A Parametric Approach

Authors: Antonio Condorelli, Sergio Petrera

Comments: 14 pages, 12 figures, submitted to PRD

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[32]  arXiv:2405.03841 (replaced) [pdf, other]

Title: Everything everywhere all at once: A detailed study of GW230529

Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash

Comments: 12 figures, 1 table, 15 pages

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

[33]  arXiv:1907.08987 (replaced) [pdf, other]

Title: Self-gravitating razor-thin disks around black holes via multi-hole seeds

Authors: Ronaldo S. S. Vieira

Comments: 24 pages, 9 figures. Published in Classical and Quantum Gravity

Journal-ref: Class. Qnatum Grav. 37, 205013 (2020)

Subjects: General Relativity and Quantum Cosmology (gr-qc); Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)

[34]  arXiv:2304.10601 (replaced) [pdf, other]

Title: The Host Galaxies of High Velocity Type Ia Supernovae

Authors: Anya E. Nugent (Northwestern/CIERA), Abigail E. Polin, Peter E. Nugent

Comments: 28 pages, 10 figures, 5 tables, submitted

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE)

[35]  arXiv:2402.08626 (replaced) [pdf, other]

Title: Constraints on Variation of the Weak Scale from Big Bang Nucleosynthesis

Authors: Anne-Katherine Burns, Venus Keus, Marc Sher, Tim M.P. Tait

Comments: Version to be published in PRD, 12 pages, 4 figures

Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Theory (nucl-th)

[36]  arXiv:2405.01887 (replaced) [pdf, other]

Title: Ab initio calculation of hyper-neutron matter

Authors: Hui Tong, Serdar Elhatisari, Ulf-G. Meißner

Comments: 17 pages, 10 figures, extended discussions, many references added

Subjects: Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Lattice (hep-lat); High Energy Physics - Phenomenology (hep-ph)

• New submissions
• Cross-lists
• Replacements